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The solar—stellar connection: the relationship between flaring rates, flare power and quiescent X-ray background

Published online by Cambridge University Press:  27 September 2017

Richard A. Harrison
Affiliation:
Astrophysics and Geophysics Division, Rutherford Appleton Laboratory
Gillian Pearce
Affiliation:
Department of Astrophysics, Oxford University, Jesus College, Oxford, and Rutherford Appleton Laboratory
Andrew Skumanich
Affiliation:
High Altitude Observatory, National Centre for Atmospheric Research (NCAR is sponsored by the National Science Foundation)

Extract

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The nature of flare activity on dMc stars (red dwarfs with strong chromospheric IIα emission lines) has been the subject of many studies. Some years ago Lacy et al. (1976) demonstrated a relationship (see also Doyle et al., 1986) between mean flare power and quiescent luminosity, in the photometric U-band. This study was extended, independently, by Skumanich (1985, 1986) and Doyle and Butler (1985) to show that the time averaged U-band power-loss due to flaring is linearly related to a star's quiescent X-ray luminosity. Skumanich also showed an inverse relationship between a star's flaring-rate and its quiescent X-ray luminosity.

Type
Session I: Stellar Flares
Copyright
Copyright © Kluwer 1989

References

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